56 Arietis
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Aries |
| Right ascension | 03h 12m 14.2461s[2] |
| Declination | +27° 15′ 25.086″[2] |
| Apparent magnitude (V) | 5.79[3] (5.75 – 5.81)[4] |
| Characteristics | |
| Spectral type | B9pSi[5] |
| U−B color index | −0.42[3] |
| B−V color index | −0.12[3] |
| Variable type | SX Ari[4] |
| Astrometry | |
| Radial velocity (Rv) | +18.0[6] km/s |
| Proper motion (μ) | RA: +11.899(94) mas/yr[2] Dec.: −18.294(88) mas/yr[2] |
| Parallax (π) | 7.8671 ± 0.0651 mas[2] |
| Distance | 415 ± 3 ly (127 ± 1 pc) |
| Absolute magnitude (MV) | +0.25[7] |
| Details | |
| Mass | 2.61[8] M☉ |
| Radius | 2.58[8] R☉ |
| Luminosity | 151[8] L☉ |
| Surface gravity (log g) | 3.97[8] cgs |
| Temperature | 12,420[8] K |
| Metallicity [Fe/H] | +0.45[9] dex |
| Rotation | 0.7278972 days[7] |
| Rotational velocity (v sin i) | 160[9] km/s |
| Age | 174[10] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
56 Arietis is a single,[12] variable star in the northern zodiac constellation of Aries. It has the variable star designation SX Arietis, while 56 Arietis is the Flamsteed designation. This object is visible to the naked eye as a faint, blue-white hued point of light with a baseline apparent visual magnitude of 5.79.[3] The estimated distance to this star is approximately 415 light-years (127 parsecs), based on parallax,[2] and it is drifting further away with a radial velocity of +18 km/s.[6]
This is a magnetic, chemically peculiar star of the silicon type with a stellar classification of B9pSi,[5] and it has a rapid rotation period of 17.5 hours.[13] This period is increasing by about two seconds every hundred years.[14] The star displays evidence of a five year period for procession of its axis.[15] Sanford S. Provin discovered that 56 Arietis is a variable star in 1952, and reported the discovery in 1953.[16] It is the prototype of a class of variable stars known as SX Arietis variables, which are rotationally variable stars with strong magnetic fields. It ranges in brightness from 5.75 down to 5.81 with a cyclical period matching its rotation rate.[4]
References
[edit]- ^ Wraight, K. T.; Fossati, L.; Netopil, M.; Paunzen, E.; Rode-Paunzen, M.; Bewsher, D.; Norton, A. J.; White, Glenn J. (February 2012). "A photometric study of chemically peculiar stars with the STEREO satellites – I. Magnetic chemically peculiar stars". Monthly Notices of the Royal Astronomical Society. 420 (1): 757–772. arXiv:1110.6283. Bibcode:2012MNRAS.420..757W. doi:10.1111/j.1365-2966.2011.20090.x. S2CID 14811051.
- ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b c d Nicolet, B. (1978), "Photoelectric photometric Catalogue of homogeneous measurements in the UBV System", Astronomy and Astrophysics Supplement Series, 34: 1–49, Bibcode:1978A&AS...34....1N.
- ^ a b c Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID 125853869.
- ^ a b Cowley, A.; et al. (April 1969), "A study of the bright A stars. I. A catalogue of spectral classifications", Astronomical Journal, 74: 375–406, Bibcode:1969AJ.....74..375C, doi:10.1086/110819
- ^ a b Bonsack, Walter K. (February 1958), "Wavelength Variations in the Spectrum of 56 ARIETIS", Publications of the Astronomical Society of the Pacific, 70 (412): 90, Bibcode:1958PASP...70...90B, doi:10.1086/127180, S2CID 122850076
- ^ a b North, P. (June 1998), "Do SI stars undergo any rotational braking?", Astronomy and Astrophysics, 334: 181–187, arXiv:astro-ph/9802286, Bibcode:1998A&A...334..181N.
- ^ a b c d e Glagolevskij, Yu. V. (2019). "On Properties of Main Sequence Magnetic Stars". Astrophysical Bulletin. 74 (1): 66. Bibcode:2019AstBu..74...66G. doi:10.1134/S1990341319010073. S2CID 149900274.
- ^ a b Ghazaryan, S.; Alecian, G.; Hakobyan, A. A. (2018). "New catalogue of chemically peculiar stars, and statistical analysis". Monthly Notices of the Royal Astronomical Society. 480 (3): 2953–2962. arXiv:1807.06902. Bibcode:2018MNRAS.480.2953G. doi:10.1093/mnras/sty1912. S2CID 119062018.
- ^ Gontcharov, G. A. (2012). "Dependence of kinematics on the age of stars in the solar neighborhood". Astronomy Letters. 38 (12): 771–782. arXiv:1606.08814. Bibcode:2012AstL...38..771G. doi:10.1134/S1063773712120031. S2CID 118345778.
- ^ "56 Ari". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-07-31.
- ^ Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
- ^ Ziznovsky, J.; et al. (January 2000), "The Variable Light Curve of 56 Arietis", Information Bulletin on Variable Stars, 4835: 1, Bibcode:2000IBVS.4835....1Z.
- ^ Sokolov, N. A. (December 2006), "Ultraviolet variability of the magnetic chemically peculiar star 56 Arietis", Monthly Notices of the Royal Astronomical Society, 373 (2): 666–676, Bibcode:2006MNRAS.373..666S, doi:10.1111/j.1365-2966.2006.11037.x.
- ^ Adelman, Saul J.; Malanushenko, V.; Ryabchikova, T. A.; Savanov, I. (September 2001), "On the rotation of the chemically peculiar magnetic star 56 Arietis", Astronomy and Astrophysics, 375 (3): 982–988, Bibcode:2001A&A...375..982A, doi:10.1051/0004-6361:20010895.
- ^ Provin, Sanford S. (September 1953). "Variation in Light of the Spectrum Variable 56 ARIETIS". Astrophysical Journal. 118: 281–284. Bibcode:1953ApJ...118..281P. doi:10.1086/145750. Retrieved 27 November 2024.
